The Gran Sasso Underground LaboratoryProgram
Eugenio CocciaINFN Gran Sasso and University of Rome “Tor Vergata”
XXXIII International Meeting on Fundamental PhysicsBenasque - March 7, 2005
Underground Laboratories
CanfrancSpain
BoulbyUK
ModaneFrance
INFN Gran Sasso National Laboratory
In 1979 A. Zichichi proposed to the Parliament the project of a large underground laboratory close to the Gran Sasso highway tunnel, then under construction
In 1982 the Parliament approved the construction, finished in 1987
In 1989 the first experiment, MACRO, started taking data
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Tunnel of 10.4 km
LNGSLNGS
L’AQUILA TERAMO
ROME
LABORATORI NAZIONALI DEL GRAN SASSO - INFN
Largest underground laboratory for astroparticle physics
1400 m rock coveragecosmic µ reduction= 10–6 (1 /m2 h)underground area: 18 000 m2
external facilitieseasy access 756 scientists from 25 countriesPermanent staff = 66 positions
Research lines• Neutrino physics (mass, oscillations, stellar physics)
• Dark matter• Nuclear reactions of astrophysics interest• Gravitational waves• Geophysics• Biology
LNGS Users
Foreigners: 356 from 24 countries
Italians: 364
Permanent Staff: 64 people
AdministrationPublic relationships supportSecretariats (visa, work permissions)OutreachEnvironmental issuesPrevention, safety, securityGeneral, safety, electrical plantsCivil worksChemistryCryogenicsMechanical shopElectronicsComputing and networksOfficesAssembly hallsLab & storage spacesLibraryConference roomsCanteen
External facilities
Evidence of neutrino oscillation
GALLEX - solar ν
MACRO - atmospheric ν
Unique cosmic ray studies
EAS-TOP with LVD
LNGS most significant results with past experiments
PRESENT EXPERIMENTS
Solar νGNOLunaBorexinoICARUS
ν fromSupernovaeLVDBorexinoICARUS
Dark MatterDAMA/LIBRA; CRESST
WARP; XENON
ν beam from CERN:ICARUSOPERA
ββ decay and rare eventsCuoricino; HDMS; GENIUS-TFCUORE; GERDA
Occupancy
Borexino
OPERA
HALL CHALL B
HALL A
LVD
CRESST2
CUORE
CUORICINO
LUNA2
DAMA
HDMSGENIUS-TF
MI R&DLUNA
COBRA
ICARUS
GERDAWARP
Gallex/GNO
101 tons Gallium Cloride solution71Ge(ve,e)71GeEnergy threshold > 233 keVSensitive mainly to pp -neutrinos
GNO Goals: measurement of the interaction rate with an accuracy of 4-5% and monitoring the neutrino flux over a complete solar cycle.
Collab.:Italy, France, Germany
SSM 115 -135 SNU
Why to perform low-energy solar neutrino experiments?[pp, 7Be, pep]
Physics and astrophysics point of view:
Test how the Sun shines. Input parameters (Z/X, opacity, …) of SSM are correct? How much energy from CNO (1.6% from SSM)? Any other energysource?
High precision neutrino flux and annual modulation determination. High precision mixing angle (θ12 ) determination [with pp].
Test of vacuum-matter transition (energy dependence of ν oscillations). Search for new physics.
CPT test by comparison with KamLAND
BOREXINO300 tons liquid scintillator in a nylon bag2200 photomultipliers2500 tons ultrapure waterEnergy threshold 0.25 MeVReal time neutrino (all flavours) detectorMeasure mono-energetic (0.86 MeV) 7Be neutrino flux through the detection of ν-e. 40 ev/d if SSM
Sphere 13.7 m diam. Supports the P�Ms & optical concentratorsSpace inside the sphere contains purified PCPurified water outside the sphere
Collab.:Italy, France, USA, Germany,
Hungary, Russia, BelgiumPoland, Canada
18 m diam., 16.9 m height
running in 2006
Borexino: how LNGS can search for low-energy solar neutrinos(only 7Be and pep)
The possibility worldwide to measure low-energy solar neutrinos in the next 2-4 yr relies on Borexino (7Be and pep) and KamLAND (only 7Be)
Assuming secular equilibriumfor internal background
Neutrino signatures and rates in Borexino:
1/R2 signature due to the eccentricity of the EarthCompton-like edge for recoil electrons from 7Beexpected ~35(54) cpd in the LMA(SSM)expected ~1(2) cpd from pep neutrinos
With a 10% measu. of 7Be the pp fluxwill be known at the level of 1%!
Borexino inner detector
BorexinoInner vessel installation
May 3, 2004
LUNA Laboratory for Underground Nuclear Astrophysics
Study of the cross section of nuclear reactions at stellar energies
in particular for pp chain 2 accelerators: 50kV - 400kV400 kV accelerator14N(p,γ)15O (CNO cycle)
50 kV accelerator3He(3He,2p)4He - D(p,γ)3He
Collab.:Italy, Germany, Hungary
Portugal
p + p → d + e+ + νe
d + p → 3He + γ
3He +3He → α + 2p 3He +4He → 7Be + γ
7Be+e-→ 7Li + γ +νe7Be + p → 8B + γ
7Li + p → α + α 8B→ 2α + e++ νe
84.7 % 13.8 %
13.78 % 0.02 %
pp chain
done in 2003
Collab.:Italy, Brazil, Russia, USA, JapanLVD Large Volume Detector
Running since 19921000 billions ν in 20s from the SN coreMeasurement of neutrinos spectra and time evolution providesimportant information on ν physics and on SN evolution.Neutrino signal detectable from SN in our Galaxy or MagellanicClouds
2 - 4 SN/century expected in our Galaxy. Plan for multidecennial observations
1000 tons liquid scintillator + layers of streamer tubes
300 ν from a SN in the center of Galaxy (8.5 kpc)SN1987A
Early warning of neutrino burst important for astronomical observations with different
messengers (Gravitational Waves)SNEWS = Supernova Early Warning System
LVD, SNO, SuperKin future: Kamland, BOREXINO
SuperSuper--Kamiokande (10Kamiokande (1044))KamlandKamland (330)(330)
SNO (800)SNO (800)MiniBooNEMiniBooNE (190)(190)
TraTra parentesiparentesi ilil numeronumerodidi eventieventi dada unauna SN alSN alcentrocentro delladella GalassiaGalassia
LVD (400)LVD (400)BorexinoBorexino (80)(80)BorexinoBorexino (80)(80)
AmandaAmandaIceCubeIceCubeIceCubeIceCube
Direct Detection Methods
Direct Detection MethodsDirect Detection Methods
DAMA Dark Matter Search
Detection of WIMPs (Weakly Interacting Massive Particle) through the flash of light produced by a Iodine nucleusrecoiling after having been hit by the WIMP.
DAMA looking for annual modulation with 100 kg NaI(Tl)
DAMA/LIBRA250 kg NaI(Tl)
Present:
Collab.:Italy, China, Ukraine
R&D in progress towardsa possible 1 ton set up
WARP: 2.3 liters prototype @ LNGSUn prototipo da 2.3 litri, equipaggiato con 7 fotomoltiplicatori, che riproduce il layout del volume sensibile centrale del rivelatoreda 100 litri proposto, è stato installatopresso i LNGS per lo studio dei fondi in galleria e dal 29 maggio è in faseoperativa.
Un rivelatore ad Argon liquido è operativopresso i Laboratori del Gran Sasso.
Emerging pictureTasks and Open QuestionsTasks and Open Questions
•• Precision for Precision for θθ12 12 andand θθ2323((θθ12 12 << 4545ºº and and θθ23 23 == 4545ºº?) ?)
•• How large is How large is θθ1313??•• CPCP--violating phaseviolating phase??•• Mass orderingMass ordering? ?
(normal (normal vsvs inverted)inverted)•• Absolute massesAbsolute masses??
(hierarchical (hierarchical vsvs degenerate)degenerate)•• DiracDirac or or MajoranaMajorana??
•• Anything beyondAnything beyond??
µµee ττ
µµee ττ
µµ ττ
11SunSun
NormalNormal
22
33
AtmosphereAtmosphere
µµee ττ
µµee ττ
µµ ττ
11SunSun
InvertedInverted
22
33
AtmosphereAtmosphere
ββ decay neutrinoless experiments
MIBETA (Milan)20 detectors of natural TeO2crystals130Te mass = 2.3 kg
CUORICINO Sensitive 130Te mass = 40 kgStatus: running
CUORE proposal presented in 2003130Te mass = 250 kg
Heidelberg-Moscow11 kg of enriched 76Ge detect.The most sensitive experiment inthe world
76Ge -->76Se + 2e-
GENIUS-TFTest facility for GENIUS40 kg HM Ge
Proposed: GERDASensitive mass: 500 kg enriched Gecrystals in Liquid N2
Collab.:Germany, Russia
Collab.:Italy, Netherland, Spain, USA
β decay n --> p + e- + ν
2β0ν is a very rare decay: T(half life) ≥ 10-25 years)
ν = ν
Majorana neutrino
Upper limit on the mass of νe 0,39 eV
CuoricinoThe CUORICINO set-up, 11 planes of 4 cristals 5x5x5 cm3 and 2 planes having 9 cristals 3x3x6 cm3 of TeO2 .The total mass is 40 kilograms, one order of magnitude bigger than other cryogenic detectorThe experiment is in data taking at Gran Sasso
With Cuore neutrino mass sensitivity < 10-2 eV(dependent from the model)
Now m < 0.4-2 eV
Neutrino masses and 0ν2β decayHeidelberg Moscow experiment
HV Klapdor et al, NIMA: Data Acquisition and Analysis of the 76-GeDouble Beta experiment in Gran Sasso 1990-2003
0.1< mν (0.4) <0.6 eV4 sigma
CNGS CERN to Gran Sasso Neutrino ProjectΑ ντ appearance program
France
Italy
Germany
Gran Sasso
CERN
Switzerland
732 Km
Austria
PS
neutrino beam
LEP -LHC
CERN
νµ beam produced at CERN and detected at LNGS after a travel of 730 km
Approved by CERN and INFN in 1999, ready in 2006
Project Overview – “Geography”
2. CNGS: the main components
vacuum
700 m 100 m 1000m 67 m
p + C → (interactions) → π+, K+, (µ+) → (decay in flight) → µ+ + νµ
Expected number of protons delivered on CNGS target:
For 1 year of CNGS operation (200 days) :
protons on target / year (“nominal”): 4.5 x 1019
Studies towards higher proton intensities in the SPS
A factor 1.5 in intensity must to be reached
CNGS schedule(schematic, simplified version)
“today”
The 2 ways of detectingτ appearance @GRAN SASSO
νµ ….. ντ → τ- + Xoscillation CC
interaction
µ- ντ νµ ΒR 18 %h- ντ nπο 50 %e- ντ νe 18 %π+ π- π- ντ nπο 14%
OPERA: Observation of the decay topology of τin photographic emulsion(~ µm granularity)
ICARUS: detailed TPC imagein liquid argon and kinematiccriteria (~ mm granularity)
Decay “kink”
ντ
ν
τ-
ν interaction
OPERA: an hybrid detector
8 cm
Emulsion analysis:VertexDecay kinke/gamma IDMultiple scattering,
kinematics
Electronic detector
→ finds the brick of νinteraction→ µ ID, charge and p Emulsions+lead + target tracker
(scintillator strips)
Spectrometer(drift tubes-RPCs)
Pb Emulsion 1 mm
Basic “cell”
OPERA CNGS (6.76 1019 pot/year in shared mode )OPERA
Ντ events 5 years data taking
0.6750.419.810.3With improvements
1.0643.817.29.0Final Design
Back∆m2 = 4.0 x 10-3∆m2 = 2.5 x 10-3∆m2 = 1.8 x 10-3
Better efficiencies due changeable sheets
Better charm background rejection with µ id. from dE/dx
P4σP3σ(%)P4σP3σ(%)
100(100)100(100)100(100)100(100)4.0x 10-3
100(100)100(100)99.6(100)100(100)3.0x 10-3
99.9(100)100(100)93.9(98.6)98.9(99.9)2.5x 10-3
99.0(99.9)99.9(100)80.5(93.0)94.9(98.9)2.2x 10-3
87.4(96.2)97.2(99.5)46.8(68.2)77.2(91.1)1.8x 10-3
5 years (33.8x 1019 pot)
3 years (20.3x 1019 pot)
∆m2(eV2)
Hall C 14 July 2003
14 October 2003
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ICARUS Imaging Cosmic and Rare Underground Signals
First Unit T600 T1200 T1200
Liquid Argon (-176 °C)Collaboration:
Italy, Poland, ChinaSpain, Switzerland, USA
First half of T600 module successfully operated in PaviaT600 underground end 2004T1800 funded
•Wide physics program •ντ and νe appearance on CNGS• atmospheric neutrinos• supernova neutrinos• solar neutrinos• proton decay 17 m
T3000 5 years 6.76 x 1019 prot/year
Signal (∆m2 = ∆∆ x 10-3 eV2)
τ Decay
∆∆ = 1.6 ∆∆ = 2.5 ∆∆ = 4.0
BG
τ e 5.5 13.5 35 1
τ ρ DIS 1 2.5 6 <0.5
τ ρ QE 1 2.5 5.5 <0.5
Total 7.5 18.5 46.5 ≤ 2
T1200T600 T1200
L’uscita dalla Sala in Pavia
ICARUS T600Dicember 3, 2004
Due criostati in Sala B
Installation of the first T600 unit at Gran Sasso
• T600 installation has started• The technical staff is working on the infrastructures in Hall B
(electrical power supply system, ventilation, heat dissipation…) • T600 will be operated in Gran Sasso at the beginning of 2006
The T600 auxiliary systemsupporting structure
5 106 km
Spacecrafts
Test Masses
Telescopes
3 pairs of “free falling” test masses
( 3 10-15 ms-2 Hz-1/2 @ 0.1 mHz)3 “test-mass follower” shielding
spacecraft
2 semi-independent 5 106 km Michelson Interferometers with
Laser Transponders
( 40 pm Hz-1/2)
Goal: GW at
0.1 mHz – 0.1 Hz
Sensitivity
4 10-21 Hz-1/2 @ 1 mHz
Theoretical activity in LNGS
the first suggestion of concept of SuperheavyDark Matter and its connection with Ultra High Energy Cosmic Rays (absence of GZK cutoff). Group of people working in UHECR under the drive of Veniamin Berezinsky
More: Neutrino physics, extensions of SM
Second phase• Upgrade of the ventilation system • Upgrade of the cooling capability• Upgrade of the electrical power
2004 - 2005 - 2006Important safety and infrastructures upgrade of the Laboratory
First phase• Floor waterproofing • Realization of containment basins • Safety measure for the drinkable water
LNGS 23 APRILE 2004
Borexino is back to workIcarus T600 is undergroundOpera is on scheduleNew ββ and DM experiments: Cuore, Gerda, Warp, Xenon GNO concluded
Upgrade of the Lab. infrastructures is in progress Relationship with local people and authorities improved
2006 crucial year
Summary of the news